File Download

There are no files associated with this item.

  Links for fulltext
     (May Require Subscription)
Supplementary

Article: The ∑ - D relation for planetary nebulae

TitleThe ∑ - D relation for planetary nebulae
Authors
KeywordsRadio continuum: ISM
Radio continuum: general
planetary nebulae: general
Methods: statistical
Methods: analytical
ISM: supernova remnants
Issue Date2009
Citation
Astronomy and Astrophysics, 2009, v. 495, n. 2, p. 537-546 How to Cite?
AbstractWe present an extended analysis of the relation between radio surface brightness and diameter - the so-called ∑ - D relation for planetary nebulae (PNe). We revise our previous derivation of the theoretical ∑ - D relation for the evolution of bremsstrahlung surface brightness in order to include the influence of the fast wind from the central star. Different theoretical forms are derived: ∑ α D-1 for the first and second phases of evolution and ∑ α D-3 for the final stage of evolution. Also, we analyzed several different Galactic PN samples. All samples are influenced by severe selection effects, but the Malmquist bias seems to be less influential here than in the supernova remnant (SNR) samples. We derived empirical ∑ - D relations for 27 sample sets using 6 updated PN papers from which an additional 21 new sets were extracted. Twenty four of these have a trivial form of β ≈ 2. However, we obtain one empirical ∑ - D relation that may be useful for determining distances to PNe. This relation is obtained by extracting a recent nearby (<1 kpc) Galactic PN sample. © 2009 ESO.
Persistent Identifierhttp://hdl.handle.net/10722/209451
ISSN
2014 Impact Factor: 4.378
2015 SCImago Journal Rankings: 2.446

 

DC FieldValueLanguage
dc.contributor.authorUrošević, D.-
dc.contributor.authorVukotić, B.-
dc.contributor.authorArbutina, B.-
dc.contributor.authorIlić, D.-
dc.contributor.authorFilipović, M.-
dc.contributor.authorBojičić, I.-
dc.contributor.authorŠegan, S.-
dc.contributor.authorVidojević, S.-
dc.date.accessioned2015-04-21T07:49:21Z-
dc.date.available2015-04-21T07:49:21Z-
dc.date.issued2009-
dc.identifier.citationAstronomy and Astrophysics, 2009, v. 495, n. 2, p. 537-546-
dc.identifier.issn0004-6361-
dc.identifier.urihttp://hdl.handle.net/10722/209451-
dc.description.abstractWe present an extended analysis of the relation between radio surface brightness and diameter - the so-called ∑ - D relation for planetary nebulae (PNe). We revise our previous derivation of the theoretical ∑ - D relation for the evolution of bremsstrahlung surface brightness in order to include the influence of the fast wind from the central star. Different theoretical forms are derived: ∑ α D-1 for the first and second phases of evolution and ∑ α D-3 for the final stage of evolution. Also, we analyzed several different Galactic PN samples. All samples are influenced by severe selection effects, but the Malmquist bias seems to be less influential here than in the supernova remnant (SNR) samples. We derived empirical ∑ - D relations for 27 sample sets using 6 updated PN papers from which an additional 21 new sets were extracted. Twenty four of these have a trivial form of β ≈ 2. However, we obtain one empirical ∑ - D relation that may be useful for determining distances to PNe. This relation is obtained by extracting a recent nearby (<1 kpc) Galactic PN sample. © 2009 ESO.-
dc.languageeng-
dc.relation.ispartofAstronomy and Astrophysics-
dc.subjectRadio continuum: ISM-
dc.subjectRadio continuum: general-
dc.subjectplanetary nebulae: general-
dc.subjectMethods: statistical-
dc.subjectMethods: analytical-
dc.subjectISM: supernova remnants-
dc.titleThe ∑ - D relation for planetary nebulae-
dc.typeArticle-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1051/0004-6361/200809494-
dc.identifier.scopuseid_2-s2.0-61549139413-
dc.identifier.volume495-
dc.identifier.issue2-
dc.identifier.spage537-
dc.identifier.epage546-
dc.identifier.eissn1432-0746-

Export via OAI-PMH Interface in XML Formats


OR


Export to Other Non-XML Formats